RAS Meeting March2019 poster - UKSSDC POSTER.pdfion propulsion thruster system throughout the 5-year...
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Determining the 3D magnetic field of the solar corona is key to answering fundamental questions about the true nature of solar atmospheric heating and solar eruptive events driving space weather at Earth. SULIS will be a flagship UK-led space science mission, which will lead a step-change in our understanding of the key physics of the Sun-Earth environment, through innovative UK-built 11U CubeSat (small-satellite) technology with industrial partnership. SULIS is now listed as 1 or 5 high priority, large-scale, fundable, solar system projects by STFC Science and Executive Board. SULIS consists of 3 pairs of formation flying coronagraphs, with one pair in a High Earth Orbit (HEO), whilst the other two pairs enter 1 AU STEREO-like Earth orbits, ahead-of and behind Earth, over a 5-year mission lifetime. SULIS will answer important questions about the 3D evolutionary properties of the magnetic field of the solar corona, at remarkably high cadence (~1-min), in order to determine the potential geo-effectiveness of Coronal Mass Ejections (CME’s) at the earliest opportunity, as well as, tracking of CME’s to determine their 3D kinematics. SULIS will compliment operational space weather missions, through exploring the science underpinning space weather sources, in order to establish better forecasting systems in future. SULIS http://sulis.space Dr Eamon Scullion (PI) 1 & Dr D Shaun Bloomfield (Northumbria University), Dr Huw Morgan (Co-PI) (Aberystwyth University), Prof Haosheng Lin (IfA, University of Hawaii, USA), Dr Jackie Davies & Prof Richard Harrison (STFC RAL Space) S olar c U besats for L inked I maging S pectropolarimetry Abstract 3D Coronal Magnetic Fields Novel Laser Optical Communications Future Project Partners 1. [email protected] Massively-multiplexed Spectropolarimetry The coronal magnetic field is one of the most important observables in the solar atmosphere, yet, one of the least explored. It is challenging to measure but critical for understanding the science underpinning Space Weather • Cononal Mass Ejections: Space weather sources are solar flares, CMEs, solar energetic particles, and geomagnetic disturbances. Knowing the north-south orientation of magnetic fields in CMEs (simulated in Figure 1) is critical for determining the potential geo-effectiveness of a CME upon impact with Earths magnetic field. The magnetic field in the corona dictates the role of MHD instabilities (such as the Kink and the Torus Instabilities) thought to drive prominence eruptions and CMEs. • Solar Flares: Energy released in solar flares s stored in the coronal magnetic field. How much energy depends on how well we can directly measure the coronal magnetic field. • Origins of Solar Wind Acceleration & Coronal Heating (waves or reconnection?): One of the longest- standing problems in solar and astro-physics concerns a) how MHD waves in the solar corona dissipate their energy leading to atmospheric heating. b) what is the role of magnetic field line braiding and reconnection in coronal loops with regard to atmospheric heating. Both wave-based phenomena and reconnection-based phenomena, across both active regions and quiet Sun, are through to be governed by the coronal magnetic field which we has never been measured across the full-disk. This is now possible with current technology. Aim of SULIS: Understand the Sun’s link to the inner heliosphere and the science underpinning space weather via revolutionary UK-led CubeSat technology. In order to accurately quantify the magnetic energy stored in the corona, we require high cadence (<1 min.), high resolution (<1 arcsec), magnetically sensitivie (<5 Gauss), continuous, direct measurement and 3D mapping of the coronal magnetic field both on-disk and off-limb. electromagnetic wave SULIS Key Objectives: 1. Provide the first direct measurements of the 3D coronal magnetic field (unique science). 2. Provide eclipse-quality imaging of the extended solar corona (out to 5 solar radii) for deeper understanding of fundamental science underpinning space weather. 3. Demonstrate UK-led future technologies (i.e, laser optical communications). Figure 1: Left Simulated EUV images of a CME in the solar corona. Right Simultaneous magnetic field line structure in the CME eruption. • Gary Lay, Business Line Director, SSTL • Prof Richard Harrison, Chief Scientist, STFC RAL Space • Dr Jackie Davies, Helio. Team Leader, STFC RAL Space • Philip Steen, Head of Technology, Andor Technology Ltd • Mark Gibbs, Head of Space Weather, UK Met Office • Prof Shadia Habbal, IfA, University of Hawaii (USA) • Prof A Ding, Technische Universitaet Berlin (Germany) • Prof Stuart Irvine, CSER, Swansea University (UK) • Dr Dan Lamb, CSER, Swansea University (UK) • Prof David Pontin, University of Dundee, (UK) • Mr Ajay Tiwari, Northumbria University (UK • Dr Matt Gunn, Aberystwyth University (UK) • Prof James McLaughlin, Northumbria University (UK) • Dr Richard Morton, Northumbria University (UK) • Dr Neil Beattie, NUPV, Northumbria University (UK) • Prof Z. Ghassemlooy, OCRG, Northumbria (UK) • Prof Mihalis Mathioudakis, Queens University Belfast (UK) • Prof Gerry Doyle, Armagh Observatory & Planetarium, (UK) • Prof Sarah Mathews, MSSL University College London (UK) • Prof Robertus Erdèlyi, University of Sheffield (UK) • Dr Viktor Fedun, University of Sheffield (UK) • Prof Valery Nakariakov, University of Warwick, UK • Dr David Long, MSSL University College London (UK) 5 solar radii Trailing CubeSat Leading CubeSat CME Formation Flying Coronagraph Trailing CubeSat Instrumentation (Coronagraphic Hyperspectral Imager): A coronagraphic high-resolution multichannel spectrometer together with a state-of-the-art broadband hyperspectral imager for observing the off-disk extended corona. An accompanying novel hyperspectral imager is included, which is linked to the development of the PanCam instrument on ExoMars (e.g. ST/G003114/1). The emission line spectra will infer electron temperatures, ion densities, bulk flow speeds and non-thermal heating, and link these to the spectropolarimeter magnetic field measurements. To provide context and high-resolution imagery, the spectrometer entrance slit is mirrored producing ‘slitjaw’ images. This system rapidly scans the visible range across the extended corona providing a spectral profile for the corona’s broadband continuum. Leading CubeSat Instrumentation (Massively-multiplexed Spectropolarimeter & Magnetometer): Bespoke 99-slit, massively-multiplexed coronal spectropolarimeter for uniquely measuring magnetic field vectors in the corona of the inner solar atmosphere. Prof Lin (PI of the DL-NIRSP instrument on DKIST) has secured $2 million of NSF funding (2018) to develop a TRL-4 prototype designed to fit into 11U CubeSat’s. The disk-imaging near-IR spectropolarimeter will be uniquely hosted on the sunward occulting CubeSat of each pair. Diffraction-grating spectrographs simultaneously observe several visible and near-IR spectral lines over multiple slits across the solar disk, as depicted in Figure 3. Inversion of the Fe XIII 1.075μm and He I 1.083μm spectra yield the magnetic field vectors through normal and saturated Hanle and Zeeman Effects. Figure 3: Left SDO/AIA synoptic observation of the solar disk from EUV channels with a grid of slit spectrometers overlaid. The Leading CubeSat’s massively multiplexed design enables rapid mastering of the full-disk (1 min cadence) for polarimetric magnetic field inversions of the near-IR spectral lines. Right Anticipated simultaneous coronagraphic observations by the occulted Trailing CubeSat instrumentation observes the corona out to 5 solar radii enabling tracking and kinematic analysis of CME eruptions in 2D or 3D (stereoscopically) The unique combination of trailing and leading CubeSat’s in each satellite pair (SULIS-A, SULIS-B and SULIS-E) results in a) ultra-low scattered light through the application of an external occulter for maximising polarimetric sensitivity and b) the opportunity to observe 3D magnetic fields off-limb and on-disk simultaneously & stereoscopically for the first time Figure 2: Top A 90 cm diameter external occulter extends (post-launch) from the sunward Leading CubeSat, resulting in an artificial eclipse falling on the anti-sunward Trailing CubeSat instrumentation, with a separation of 100 m. The pair of CubeSat’s will fly in formation maintaining positioning via an ion propulsion thruster system throughout the 5- year mission lifetime. Uniquely, the Leading CubeSat serves as an occulter, as well as, housing instrumentation for solar observations. Bottom: The 3D magnetic field and kinematic properties of a CME from the Sun can be tracked through the combination of synchronous observations from 3 pairs of CubeSat’s flying in formation, along the Earth orbit. Each CubeSat pair is referred to as SULIS-A, SULIS-B and SULIS-E. The UK Met Office is a key stakeholder in the SULIS mission concept. Figure 4: Li-Fi has the potential to revolutionise satellite-to-satellite and satellite-to-ground communications. A key aspect of the SULIS mission will be the technology demonstration of Li-Fi (note: a similar demonstration was proposed in the ESA-DOCS and INSTANT mission concepts). External Occulter Coronagraph SULIS offers bespoke UK technology demonstration with a wide range of applications, benefitting society and industry across many sectors Next-generation Power-by-light Optical Wireless Communications (OWC) technology will be demonstrated in space for the first time. The demand for high-speed internet services has driven emergent technologies capable of delivering ultra-high data rates to end users. SULIS will demonstrate optical power transmission (offering mark-up data transfer rates compared with X-band antenna transmission) characteristic of Power-by-Light systems, an elegant method for powering PV solar cells across large distances, using laser light (aka Li-Fi). Li-Fi can also achieve very precise alignment of formation-flying smart CubeSat’s, important for maintaining a precise satellite alignment for a functioning coronagraph. SULIS will demonstrate autonomous CubeSat clusters which self-consistently control proximity satellite manoeuvres. This is of substantial interest within the international spaceflight community, e.g., the AAREST mission highlights the need for enabling technology for assembly of future large space telescopes. Li-Fi is the future of communications technology (Northumbria University): Li-Fi communication will rapidly redistribute the data between CubeSat pairs (i.e. SULIS-A & B), before transmission to SULIS-E at ~100 Mbps each. In 2001, a 50 Mbps link was successfully established between the ARTEMIS geostationary satellite and the SPOT-4 satellite. SULIS-E will also redistribute data and provide a downlink transfer at ~600 Mbps, as depicted in Figure 4. In 2013, NASA’s lunar laser communication demonstration achieved an impressive downlink rate of 622 Mbps. The application of high-speed data transfer using light is highly advantageous for SULIS given that Li-Fi significantly reduces the payload mass. Li-Fi technology is a novel solution for 1) limited CubeSat bandwidth (Li-Fi offers expansive bandwidth) 2) connectivity (Li-Fi is highly energy efficient in monochromatic laser light) and 3) range (Li-Fi can transfer ethernet internet speeds). SULIS CubeSat construction will be managed by industrial partners SSTL. SSTL delivers complete mission solutions for remote sensing, science, exploration, navigation and telecommunications. The ground station segment for mission operations will be supported by STFC-RAL Space in collaboration with SSTL. Clusters of small ~15 cm telescopes (suitable for 11U CubeSat’s) operating collectively can achieve the same magnetic field sensitivity as a large ~1 m telescope, but at a significant cost saving. The technological innovations of SULIS will advance the power efficiency, communications and control for CubeSat’s and small- satellite constellations in general. To properly determine the magnetic field of the solar corona, single-viewpoint Coronal Emission Line Spectropolarimetry (CELS) is not enough. We require multiple-viewpoint CELS with a large separation angle for disambiguation of the plane-of-sky coronal magnetic field vectors. Utilising the collective power of space-based stereoscopy (depicted in Figure 2 Bottom), employing CELS from instruments housed in pairs of CubeSat’s (depicted in Figure 2 Top) makes up SULIS (combining 3 pairs: SULIS-Ahead, SULIS-Behind and SULIS-Earth) will enable reconstruction of the 3D coronal magnetic field in real-time. SULIS will build-on and demonstrate the strength and legacy of UK space leadership • SULIS provides an exciting opportunity to strengthen the collaborative relationship between STFC and the UK space industry. The UK’s growing space sector is a core part of the UK government Industrial Strategy. • SULIS compliments operational space weather missions (e.g ESAs potential L5 mission, NASA’s L1 follow-on to DISCOVR and the ASPIICS/PROBA-3) paving the way for future space weather instruments. All partner organisations have established public outreach programmes and will promote SULIS and raise public awareness of space weather hazards. • SULIS is ambitious, yet risk is mitigated through the initial launch of SULIS-E, followed by SULIS-A & B, 1–2 years later. Limiting the initial mission to one pair will first test the feasibility of the formation-flying coronagraph. SULIS-E
Transcript of RAS Meeting March2019 poster - UKSSDC POSTER.pdfion propulsion thruster system throughout the 5-year...
Determining the 3D magnetic field of the solar corona is key to answering fundamental questions about the true nature of solar atmospheric heating and solar eruptive events driving space weather at Earth. SULIS will be a flagship UK-led space science mission, which will lead a step-change in our understanding of the key physics of the Sun-Earth environment, through innovative UK-built 11U CubeSat (small-satellite) technology with industrial partnership. SULIS is now listed as 1 or 5 high priority, large-scale, fundable, solar system projects by STFC Science and Executive Board. SULIS consists of 3 pairs of formation flying coronagraphs, with one pair in a High Earth Orbit (HEO), whilst the other two pairs enter 1 AU STEREO-like Earth orbits, ahead-of and behind Earth, over a 5-year mission lifetime. SULIS will answer important questions about the 3D evolutionary properties of the magnetic field of the solar corona, at remarkably high cadence (~1-min), in order to determine the potential geo-effectiveness of Coronal Mass Ejections (CME’s) at the earliest opportunity, as well as, tracking of CME’s to determine their 3D kinematics. SULIS will compliment operational space weather missions, through exploring the science underpinning space weather sources, in order to establish better forecasting systems in future.
SULIShttp://sulis.space
Dr Eamon Scullion (PI) 1 & Dr D Shaun Bloomfield (Northumbria University), Dr Huw Morgan (Co-PI) (Aberystwyth University), Prof Haosheng Lin (IfA, University of Hawaii, USA), Dr Jackie Davies & Prof Richard Harrison (STFC RAL Space)
Solar cUbesats for Linked Imaging Spectropolarimetry
Abstract
3D Coronal Magnetic Fields
Novel Laser Optical Communications
Future Project Partners
Massively-multiplexed Spectropolarimetry
The coronal magnetic field is one of the most important observables in the solar atmosphere, yet, one of the least explored. It is challenging to measure but critical for understanding
the science underpinning Space Weather
• Cononal Mass Ejections: Space weather sources are solar flares, CMEs, solar energetic particles, and geomagnetic disturbances. Knowing the north-south orientation of magnetic fields in CMEs (simulated in Figure 1) is critical for determining the potential geo-effectiveness of a CME upon impact with Earths magnetic field. The magnetic field in the corona dictates the role of MHD instabilities (such as the Kink and the Torus Instabilities) thought to drive prominence eruptions and CMEs.
• Solar Flares: Energy released in solar flares s stored in the coronal magnetic field. How much energy depends on how well we can directly measure the coronal magnetic field.
• Origins of Solar Wind Acceleration & Coronal Heating (waves or reconnection?): One of the longest-standing problems in solar and astro-physics concerns a) how MHD waves in the solar corona dissipate their energy leading to atmospheric heating. b) what is the role of magnetic field line braiding and reconnection in coronal loops with regard to atmospheric heating. Both wave-based phenomena and reconnection-based phenomena, across both active regions and quiet Sun, are through to be governed by the coronal magnetic field which we has never been measured across the full-disk. This is now possible with current technology.
Aim of SULIS: Understand the Sun’s link to the inner heliosphere and the science underpinning space weather via revolutionary UK-led CubeSat technology. In order to accurately quantify the magnetic energy stored in the corona, we require high cadence (<1 min.), high resolution (<1 arcsec), magnetically sensitivie (<5 Gauss), continuous, direct measurement and 3D mapping of the coronal magnetic field both on-disk and off-limb.
electromagnetic wave
SULIS Key Objectives:1.Provide the first direct measurements of the
3D coronal magnetic field (unique science).
2.Provide eclipse-quality imaging of the extended solar corona (out to 5 solar radii) for deeper understanding of fundamental science underpinning space weather.
3.Demonstrate UK-led future technologies (i.e, laser optical communications).
Figure 1: Left Simulated EUV images of a CME in the solar corona. Right Simultaneous magnetic field line structure in the CME eruption.
•Gary Lay, Business Line Director, SSTL•Prof Richard Harrison, Chief Scientist, STFC RAL Space•Dr Jackie Davies, Helio. Team Leader, STFC RAL Space•Philip Steen, Head of Technology, Andor Technology Ltd•Mark Gibbs, Head of Space Weather, UK Met Office•Prof Shadia Habbal, IfA, University of Hawaii (USA)•Prof A Ding, Technische Universitaet Berlin (Germany)•Prof Stuart Irvine, CSER, Swansea University (UK)•Dr Dan Lamb, CSER, Swansea University (UK)•Prof David Pontin, University of Dundee, (UK)•Mr Ajay Tiwari, Northumbria University (UK•Dr Matt Gunn, Aberystwyth University (UK)
•Prof James McLaughlin, Northumbria University (UK)•Dr Richard Morton, Northumbria University (UK)•Dr Neil Beattie, NUPV, Northumbria University (UK)•Prof Z. Ghassemlooy, OCRG, Northumbria (UK)•Prof Mihalis Mathioudakis, Queens University Belfast (UK)•Prof Gerry Doyle, Armagh Observatory & Planetarium, (UK)•Prof Sarah Mathews, MSSL University College London (UK)•Prof Robertus Erdèlyi, University of Sheffield (UK)•Dr Viktor Fedun, University of Sheffield (UK)•Prof Valery Nakariakov, University of Warwick, UK•Dr David Long, MSSL University College London (UK)
5 solar radii
Trailing CubeSat
Leading CubeSat
CME
Formation Flying Coronagraph
Trailing CubeSat Instrumentation (Coronagraphic Hyperspectral Imager): A coronagraphic high-resolution multichannel spectrometer together with a state-of-the-art broadband hyperspectral imager for observing the off-disk extended corona. An accompanying novel hyperspectral imager is included, which is linked to the development of the PanCam instrument on ExoMars (e.g. ST/G003114/1). The emission line spectra will infer electron temperatures, ion densities, bulk flow speeds and non-thermal heating, and link these to the spectropolarimeter magnetic field measurements. To provide context and high-resolution imagery, the spectrometer entrance slit is mirrored producing ‘slitjaw’ images. This system rapidly scans the visible range across the extended corona providing a spectral profile for the corona’s broadband continuum.
Leading CubeSat Instrumentation (Massively-multiplexed Spectropolarimeter & Magnetometer): Bespoke 99-slit, massively-multiplexed coronal spectropolarimeter for uniquely measuring magnetic field vectors in the corona of the inner solar atmosphere. Prof Lin (PI of the DL-NIRSP instrument on DKIST) has secured $2 million of NSF funding (2018) to develop a TRL-4 prototype designed to fit into 11U CubeSat’s. The disk-imaging near-IR spectropolarimeter will be uniquely hosted on the sunward occulting CubeSat of each pair. Diffraction-grating spectrographs simultaneously observe several visible and near-IR spectral lines over multiple slits across the solar disk, as depicted in Figure 3. Inversion of the Fe XIII 1.075µm and He I 1.083µm spectra yield the magnetic field vectors through normal and saturated Hanle and Zeeman Effects.
Figure 3: Left SDO/AIA synoptic observation of the solar disk from EUV channels with a grid of slit spectrometers overlaid. The Leading CubeSat’s massively multiplexed design enables rapid mastering of the full-disk (1 min cadence) fo r po la r imet r i c magnetic field inversions of the near-IR spectral lines. Right Anticipated simultaneous coronagraphic observations by the occulted Trailing CubeSat instrumentation observes the corona out to 5 solar radii enabling tracking and kinematic analysis of CME eruptions in 2D or 3D (stereoscopically)
The unique combination of trailing and leading CubeSat’s in each satellite pair (SULIS-A, SULIS-B and SULIS-E) results in a) ultra-low scattered light through the application of an
external occulter for maximising polarimetric sensitivity and b) the opportunity to observe 3D magnetic fields off-limb and on-disk simultaneously & stereoscopically for the first time
Figure 2: Top A 90 cm diameter external occulter extends (post-launch) from the sunward Leading CubeSat, resulting in an artificial eclipse falling on the anti-sunward Trailing CubeSat instrumentation, with a separation of 100 m. The pair of CubeSat’s will fly in formation maintaining positioning via an ion propulsion thruster system throughout the 5-year mission lifetime. Uniquely, the Leading CubeSat serves as an occulter, as well as, housing instrumentation for solar observations.Bottom: The 3D magnetic field and kinematic properties of a CME from the Sun can be tracked through the combination of synchronous observations from 3 pairs of CubeSat’s flying in formation, along the Earth orbit. Each CubeSat pair is referred to as SULIS-A, SULIS-B and SULIS-E. The UK Met Office is a key stakeholder in the SULIS mission concept.
Figure 4: Li-Fi has the potential to revolutionise satellite-to-satellite and satellite-to-ground communications. A key aspect of the SULIS mission will be the technology demonstration of Li-Fi (note: a similar demonstration was proposed in the ESA-DOCS and INSTANT mission concepts).
External Occulter Coronagraph
SULIS offers bespoke UK technology demonstration with a wide range of applications, benefitting society and industry across many sectors
Next-generation Power-by-light Optical Wireless Communications (OWC) technology will be demonstrated in space for the first time. The demand for high-speed internet services has driven emergent technologies capable of delivering ultra-high data rates to end users. SULIS will demonstrate optical power transmission (offering mark-up data transfer rates compared with X-band antenna transmission) characteristic of Power-by-Light systems, an elegant method for powering PV solar cells across large distances, using laser light (aka Li-Fi). Li-Fi can also achieve very precise alignment of formation-flying smart CubeSat’s, important for maintaining a precise satellite alignment for a functioning coronagraph. SULIS will demonstrate autonomous CubeSat clusters which self-consistently control proximity satellite manoeuvres. This is of substantial interest within the international spaceflight community, e.g., the AAREST mission highlights the need for enabling technology for assembly of future large space telescopes.
Li-Fi is the future of communications technology (Northumbria University): Li-Fi communication will rapidly redistribute the data between CubeSat pairs (i.e. SULIS-A & B), before transmission to SULIS-E at ~100 Mbps each. In 2001, a 50 Mbps link was successfully established between the ARTEMIS geostationary satellite and the SPOT-4 satellite. SULIS-E will also redistribute data and provide a downlink transfer at ~600 Mbps, as depicted in Figure 4. In 2013, NASA’s lunar laser communication demonstration achieved an impressive downlink rate of 622 Mbps. The application of high-speed data transfer using light is highly advantageous for SULIS given that Li-Fi significantly reduces the payload mass. Li-Fi technology is a novel solution for 1) limited CubeSat bandwidth (Li-Fi offers expansive bandwidth) 2) connectivity (Li-Fi is highly energy efficient in monochromatic laser light) and 3) range (Li-Fi can transfer ethernet internet speeds).
SULIS CubeSat construction will be managed by industrial partners SSTL. SSTL delivers complete mission solutions for remote sensing, science, exploration, navigation and telecommunications. The ground station segment for mission operations will be supported by STFC-RAL Space in collaboration with SSTL.
Clusters of small ~15 cm telescopes (suitable for 11U CubeSat’s) operating collectively can achieve the same magnetic field sensitivity as a large ~1 m telescope, but at a significant cost saving. The technological innovations of SULIS will advance the power efficiency, communications and control for CubeSat’s and small-satellite constellations in general.
To properly determine the magnetic field of the solar corona, single-viewpoint Coronal Emission Line Spectropolarimetry (CELS) is not enough. We require multiple-viewpoint CELS with a large separation angle for disambiguation of the plane-of-sky coronal magnetic field vectors. Utilising the collective power of space-based stereoscopy (depicted in Figure 2 Bottom), employing CELS from instruments housed in pairs of CubeSat’s (depicted in Figure 2 Top) makes up SULIS (combining 3 pairs: SULIS-Ahead, SULIS-Behind and SULIS-Earth) will enable reconstruction of the 3D coronal magnetic field in real-time.
SULIS will build-on and demonstrate the strength and legacy of UK space leadership
•SULIS provides an exciting opportunity to strengthen the collaborative relationship between STFC and the UK space industry. The UK’s growing space sector is a core part of the UK government Industrial Strategy.
•SULIS compliments operational space weather missions (e.g ESAs potential L5 mission, NASA’s L1 follow-on to DISCOVR and the ASPIICS/PROBA-3) paving the way for future space weather instruments. All partner organisations have established public outreach programmes and will promote SULIS and raise public awareness of space weather hazards.
•SULIS is ambitious, yet risk is mitigated through the initial launch of SULIS-E, followed by SULIS-A & B, 1–2 years later. Limiting the initial mission to one pair will first test the feasibility of the formation-flying coronagraph.
SULIS-E
